382:. For sufficiently high temperatures, such as those existing in the early Universe, the dark matter particle and its antiparticle would have been both forming from and annihilating into lighter particles. As the Universe expanded and cooled, the average thermal energy of these lighter particles decreased and eventually became insufficient to form a dark matter particle-antiparticle pair. The annihilation of the dark matter particle-antiparticle pairs, however, would have continued, and the number density of dark matter particles would have begun to decrease exponentially. Eventually, however, the number density would become so low that the dark matter particle and antiparticle interaction would cease, and the number of dark matter particles would remain (roughly) constant as the Universe continued to expand. Particles with a larger interaction cross section would continue to annihilate for a longer period of time, and thus would have a smaller number density when the annihilation interaction ceases. Based on the current estimated abundance of dark matter in the Universe, if the dark matter particle is such a relic particle, the interaction cross section governing the particle-antiparticle annihilation can be no larger than the cross section for the weak interaction. If this model is correct, the dark matter particle would have the properties of the WIMP.
4612:
682:(CCDs) to detect light Dark Matter. The CCDs act as both the detector target and the readout instrumentation. WIMP interactions with the bulk of the CCD can induce the creation of electron-hole pairs, which are then collected and readout by the CCDs. In order to decrease the noise and achieve detection of single electrons, the experiments make use of a type of CCD known as the Skipper CCD, which allows for averaging over repeated measurements of the same collected charge.
474:
4684:
4572:
729:, a smaller detector using a single germanium puck, designed to sense WIMPs with smaller masses, reported hundreds of detection events in 56 days. They observed an annual modulation in the event rate that could indicate light dark matter. However a dark matter origin for the CoGeNT events has been refuted by more recent analyses, in favour of an explanation in terms of a background from surface events.
4648:
3980:
4672:
4584:
4624:
4660:
4636:
419:-LAT gamma ray telescope and the VERITAS ground-based gamma ray observatory. Although the annihilation of WIMPs into Standard Model particles also predicts the production of high-energy neutrinos, their interaction rate is thought to be too low to reliably detect a dark matter signal at present. Future observations from the
466:
remains possible that these models are either incorrect or only explain part of the dark matter phenomenon. Thus, even with the multiple experiments dedicated to providing indirect evidence for the existence of cold dark matter, direct detection measurements are also necessary to solidify the theory of WIMPs.
638:
advantage of the bubble detector technique is that the detector is almost insensitive to background radiation. The detector sensitivity can be adjusted by changing the temperature, typically operated between 15 °C and 55 °C. There is another similar experiment using this technique in Europe called
740:
collaboration (a merging of KIMS and DM-Ice groups) published their results on replicating the DAMA/LIBRA signal in
December 2018 in journal Nature; their conclusion was that "this result rules out WIMP–nucleon interactions as the cause of the annual modulation observed by the DAMA collaboration". In
707:
experiments, as shown in figure 2. With 370 kilograms of xenon LUX is more sensitive than XENON or CDMS. First results from
October 2013 report that no signals were seen, appearing to refute results obtained from less sensitive instruments. and this was confirmed after the final data run ended in May
762:
The 2020s should see the emergence of several multi-tonne mass direct detection experiments, which will probe WIMP-nucleus cross sections orders of magnitude smaller than the current state-of-the-art sensitivity. Examples of such next-generation experiments are LUX-ZEPLIN (LZ) and XENONnT, which are
341:
Because of their lack of electromagnetic interaction with normal matter, WIMPs would be invisible through normal electromagnetic observations. Because of their large mass, they would be relatively slow moving and therefore "cold". Their relatively low velocities would be insufficient to overcome the
766:
Such multi-tonne experiments will also face a new background in the form of neutrinos, which will limit their ability to probe the WIMP parameter space beyond a certain point, known as the neutrino floor. However, although its name may imply a hard limit, the neutrino floor represents the region of
732:
Annual modulation is one of the predicted signatures of a WIMP signal, and on this basis the DAMA collaboration has claimed a positive detection. Other groups, however, have not confirmed this result. The CDMS data made public in May 2004 exclude the entire DAMA signal region given certain standard
645:
PICASSO reports results (November 2009) for spin-dependent WIMP interactions on F, for masses of 24 Gev new stringent limits have been obtained on the spin-dependent cross section of 13.9 pb (90% CL). The obtained limits restrict recent interpretations of the DAMA/LIBRA annual modulation effect in
465:
refers to the observation of the effects of a WIMP-nucleus collision as the dark matter passes through a detector in an Earth laboratory. While most WIMP models indicate that a large enough number of WIMPs must be captured in large celestial bodies for indirect detection experiments to succeed, it
694:
Figure 2: Plot showing the parameter space of dark matter particle mass and interaction cross section with nucleons. The LUX and SuperCDMS limits exclude the parameter space above the labelled curves. The CoGeNT and CRESST-II regions indicate regions which were previously thought to correspond to
2164:
Abramoff, Orr; Barak, Liron; Bloch, Itay M.; Chaplinsky, Luke; Crisler, Michael; Dawa; Drlica-Wagner, Alex; Essig, Rouven; Estrada, Juan; Etzion, Erez; Fernandez, Guillermo (2019-04-24). "SENSEI: Direct-Detection
Constraints on Sub-GeV Dark Matter from a Shallow Underground Run Using a Prototype
637:
at a time, the detector can stay active for much longer periods. When enough energy is deposited in a droplet by ionizing radiation, the superheated droplet becomes a gas bubble. The bubble development is accompanied by an acoustic shock wave that is picked up by piezo-electric sensors. The main
469:
Although most WIMPs encountering the Sun or the Earth are expected to pass through without any effect, it is hoped that a large number of dark matter WIMPs crossing a sufficiently large detector will interact often enough to be seen—at least a few events per year. The general strategy of current
1905:
Behnke, E.; Behnke, J.; Brice, S. J.; Broemmelsiek, D.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Fustin, D.; Hall, J.; Hinnefeld, J. H.; Hu, M.; Levine, I.; Ramberg, E.; Shepherd, T.; Sonnenschein, A.; Szydagis, M. (10 January 2011). "Improved Limits on Spin-Dependent WIMP-Proton
370:
A decade after the dark matter problem was established in the 1970s, WIMPs were suggested as a potential solution to the issue. Although the existence of WIMPs in nature is still hypothetical, it would resolve a number of astrophysical and cosmological problems related to dark matter. There is
745:
both failed to replicate the DAMA/LIBRA signal and in August 2022 COSINE-100 applied an analysis method similar to one used by DAMA/LIBRA and found a similar annual modulation suggesting the signal could be just a statistical artifact supporting a hypothesis first put forward in 2020.
401:
refers to the observation of annihilation or decay products of WIMPs far away from Earth. Indirect detection efforts typically focus on locations where WIMP dark matter is thought to accumulate the most: in the centers of galaxies and galaxy clusters, as well as in the smaller
415:. The spectrum and intensity of a gamma ray signal depends on the annihilation products, and must be computed on a model-by-model basis. Experiments that have placed bounds on WIMP annihilation, via the non-observation of an annihilation signal, include the
427:
Another type of indirect WIMP signal could come from the Sun. Halo WIMPs may, as they pass through the Sun, interact with solar protons, helium nuclei as well as heavier elements. If a WIMP loses enough energy in such an interaction to fall below the local
3607:
LUX-ZEPLIN Collaboration; Aalbers, J.; Akerib, D. S.; Akerlof, C. W.; Al
Musalhi, A. K.; Alder, F.; Alqahtani, A.; Alsum, S. K.; Amarasinghe, C. S.; Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M. (2023-07-28).
559:
used xenon to exclude WIMPs at higher sensitivity, with the most stringent limits to date provided by the XENON1T detector, utilizing 3.5 tons of liquid xenon. Even larger multi-ton liquid xenon detectors have been approved for construction from the
767:
parameter space beyond which experimental sensitivity can only improve at best as the square root of exposure (the product of detector mass and running time). For WIMP masses below 10 GeV the dominant source of neutrino background is from the
162:
501:. A layer of metal (aluminium and tungsten) at the surfaces is used to detect a WIMP passing through the crystal. This design hopes to detect vibrations in the crystal matrix generated by an atom being "kicked" by a WIMP. The tungsten
3541:
XENON Collaboration; Aprile, E.; Abe, K.; Agostini, F.; Ahmed
Maouloud, S.; Althueser, L.; Andrieu, B.; Angelino, E.; Angevaare, J. R.; Antochi, V. C.; Antón Martin, D.; Arneodo, F.; Baudis, L.; Baxter, A. L.; Bazyk, M. (2023-07-28).
371:
consensus today among astronomers that most of the mass in the
Universe is indeed dark. Simulations of a universe full of cold dark matter produce galaxy distributions that are roughly similar to what is observed. By contrast,
423:
observatory in
Antarctica may be able to differentiate WIMP-produced neutrinos from standard astrophysical neutrinos; however, by 2014, only 37 cosmological neutrinos had been observed, making such a distinction impossible.
695:
dark matter signals, but which were later explained with mundane sources. The DAMA and CDMS-Si data remain unexplained, and these regions indicate the preferred parameter space if these anomalies are due to dark matter.
406:
of the Milky Way. These are particularly useful since they tend to contain very little baryonic matter, reducing the expected background from standard astrophysical processes. Typical indirect searches look for excess
396:
Because WIMPs may only interact through gravitational and weak forces, they would be extremely difficult to detect. However, there are many experiments underway to attempt to detect WIMPs both directly and indirectly.
470:
attempts to detect WIMPs is to find very sensitive systems that can be scaled to large volumes. This follows the lessons learned from the history of the discovery, and (by now routine) detection, of the neutrino.
2098:
DAMIC Collaboration; Aguilar-Arevalo, A.; Amidei, D.; Baxter, D.; Cancelo, G.; Cervantes
Vergara, B. A.; Chavarria, A. E.; Darragh-Ford, E.; de Mello Neto, J. R. T.; D’Olivo, J. C.; Estrada, J. (2019-10-31).
432:, it would theoretically not have enough energy to escape the gravitational pull of the Sun and would remain gravitationally bound. As more and more WIMPs thermalize inside the Sun, they would begin to
4194:
514:
3027:
Adhikari, G.; Carlin, N.; Choi, J. J.; Choi, S.; Ezeribe, A. C.; Franca, L. E.; Ha, C.; Hahn, I. S.; Hollick, S. J.; Jeon, E. J.; Jo, J. H.; Joo, H. W.; Kang, W. G.; Kauer, M.; Kim, B. H. (2023).
2928:
Adhikari, Govinda; de Souza, Estella B.; Carlin, Nelson; Choi, Jae Jin; Choi, Seonho; Djamal, Mitra; Ezeribe, Anthony C.; França, Luis E.; Ha, Chang Hyon; Hahn, In Sik; Jeon, Eunju (2021-11-12).
622:
as the active mass. PICASSO is predominantly sensitive to spin-dependent interactions of WIMPs with the fluorine atoms in the Freon. COUPP, a similar experiment using trifluoroiodomethane(CF
63:, but also non-vanishing in strength. Many WIMP candidates are expected to have been produced thermally in the early Universe, similarly to the particles of the Standard Model according to
1477:
Ackermann, M.; et al. (The Fermi-LAT Collaboration) (2014). "Dark matter constraints from observations of 25 Milky Way satellite galaxies with the Fermi Large Area
Telescope".
1131:
Klapdor-Kleingrothaus, H. V. (1998). "Double beta decay and dark matter search – window to new physics now, and in future (GENIUS)". In
Klapdor-Kleingrothaus, V.; Paes, H. (eds.).
1467:
The Millennium Run used more than 10 billion particles to trace the evolution of the matter distribution in a cubic region of the Universe over 2 billion light-years on a side.
3264:
Billard, J.; Strigari, L.; Figueroa-Feliciano, E. (2014). "Implication of neutrino backgrounds on the reach of next generation dark matter direct detection experiments".
4279:
4259:
85:
2863:
Amaré, J.; Cebrián, S.; Cintas, D.; Coarasa, I.; García, E.; Martínez, M.; Oliván, M. A.; Ortigoza, Y.; de Solórzano, A. Ortiz; Puimedón, J.; Salinas, A. (2021-05-27).
2849:
868:
3798:
Del Nobile, Eugenio; Gelmini, Graciela B.; Gondolo, Paolo; Huh, Ji-Haeng (2015). "Update on the Halo-independent Comparison of Direct Dark Matter Detection Data".
4249:
660:
629:
A bubble detector is a radiation sensitive device that uses small droplets of superheated liquid that are suspended in a gel matrix. It uses the principle of a
354:. These names were deliberately chosen for contrast, with MACHOs named later than WIMPs. In contrast to WIMPs, there are no known stable particles within the
3370:
Meng, Yue; Wang, Zhou; Tao, Yi; Abdukerim, Abdusalam; Bo, Zihao; Chen, Wei; Chen, Xun; Chen, Yunhua; Cheng, Chen; Cheng, Yunshan; Cui, Xiangyi (2021-12-23).
2549:
C. E. Aalseth; et al. (CoGeNT collaboration) (2011). "Results from a Search for Light-Mass Dark Matter with a P-type Point Contact Germanium Detector".
711:
Historically there have been four anomalous sets of data from different direct detection experiments, two of which have now been explained with backgrounds (
4174:
1644:
Ferrer, F.; Krauss, L. M.; Profumo, S. (2006). "Indirect detection of light neutralino dark matter in the next-to-minimal supersymmetric standard model".
444:
detector in Japan. The number of neutrino events detected per day at these detectors depends on the properties of the WIMP, as well as on the mass of the
4709:
238:
of particle physics, although none of the large number of new particles in supersymmetry have been observed. WIMP-like particles are also predicted by
4432:
1967:
206:
extensions of the Standard Model of particle physics readily predict a new particle with these properties, this apparent coincidence is known as the "
691:
4437:
4412:
578:– Instead of a liquid noble gas, an in principle simpler approach is the use of a scintillating crystal such as NaI(Tl). This approach is taken by
699:
There are currently no confirmed detections of dark matter from direct detection experiments, with the strongest exclusion limits coming from the
1583:
Aartsen, M. G.; et al. (IceCube Collaboration) (2014). "Observation of High-Energy Astrophysical Neutrinos in Three Years of IceCube Data".
3853:
3317:
Davis, Jonathan H. (2015). "Dark Matter vs. Neutrinos: The effect of astrophysical uncertainties and timing information on the neutrino floor".
678:
The DAMIC (DArk Matter In CCDs) and SENSEI (Sub Electron Noise Skipper CCD Experimental Instrument) collaborations employ the use of scientific
448:. Similar experiments are underway to attempt to detect neutrinos from WIMP annihilations within the Earth and from within the galactic center.
4611:
3859:
755:
671:
readout plane that allows it to be reconstructed in three dimensions and determine the origin direction. DMTPC is a similar experiment with CF
4029:
3904:
3696:
1233:
776:
733:
assumptions about the properties of the WIMPs and the dark matter halo, and this has been followed by many other experiments (see Figure 2).
411:, which are predicted both as final-state products of annihilation, or are produced as charged particles interact with ambient radiation via
4387:
4117:
723:). In February 2010, researchers at CDMS announced that they had observed two events that may have been caused by WIMP-nucleus collisions.
667:
target, that allows WIMP recoils to travel several millimetres, leaving a track of charged particles. This charged track is drifted to an
342:
mutual gravitational attraction, and as a result, WIMPs would tend to clump together. WIMPs are considered one of the main candidates for
4244:
556:
548:
497:
relies on multiple very cold germanium and silicon crystals. The crystals (each about the size of a hockey puck) are cooled to about 50
2611:
2290:
1411:
Conroy, Charlie; Wechsler, Risa H.; Kravtsov, Andrey V. (2006). "Modeling Luminosity-Dependent Galaxy Clustering Through Cosmic Time".
4269:
763:
multi-tonne liquid xenon experiments, followed by DARWIN, another proposed liquid xenon direct detection experiment of 50–100 tonnes.
700:
2234:
4224:
3733:
544:
391:
4009:
893:
614:(Project In Canada to Search for Supersymmetric Objects) experiment is a direct dark matter search experiment that is located at
273:
4724:
4417:
4407:
4392:
4329:
457:
416:
358:
of particle physics that have the properties of MACHOs. The particles that have little interaction with normal matter, such as
4714:
4537:
758:
Upper limits for WIMP-nucleon elastic cross sections from selected experiments as reported by the LZ experiment in July 2023.
4402:
2633:
Davis, Jonathan H.; McCabe, Christopher; Boehm, Celine (2014). "Quantifying the evidence for Dark Matter in CoGeNT data".
2437:
4602:
4729:
4422:
4339:
4289:
4169:
4164:
4149:
3959:
3846:(S. Eidelman et al. (Particle Data Group), Physical Letters B 592, 1 (2004) Appendix : OMITTED FROM SUMMARY TABLE).
840:
720:
704:
597:
490:
347:
2788:
COSINE-100 Collaboration (2018). "An experiment to search for dark-matter interactions using sodium iodide detectors".
210:", and a stable supersymmetric partner has long been a prime WIMP candidate. However, in the early 2010s, results from
4377:
4264:
4204:
4184:
4107:
2412:
852:
737:
601:
1047:
187:
in nearby galaxies and galaxy clusters; direct detection experiments designed to measure the collision of WIMPs with
4397:
2686:
Drukier, Andrzej K.; Freese, Katherine; Spergel, David N. (15 June 1986). "Detecting cold dark-matter candidates".
535:
material, so that light pulses are generated by the moving atom and detected, often with PMTs. Experiments such as
412:
378:
WIMPs fit the model of a relic dark matter particle from the early Universe, when all particles were in a state of
440:. These neutrinos may then travel to the Earth to be detected in one of the many neutrino telescopes, such as the
4102:
3897:
281:
239:
1530:
Grube, Jeffrey; VERITAS Collaboration (2012). "VERITAS Limits on Dark Matter Annihilation from Dwarf Galaxies".
626:
I), published limits for mass above 20 GeV in 2011. The two experiments merged into PICO collaboration in 2012.
4122:
3964:
375:
would smear out the large-scale structure of galaxies and thus is not considered a viable cosmological model.
3003:
663:(DRIFT) collaboration is attempting to utilize the predicted directionality of the WIMP signal. DRIFT uses a
4087:
4039:
878:
656:
502:
323:
79:
4588:
1971:
4719:
509:
state. Large crystal vibrations will generate heat in the metal and are detectable because of a change in
31:
2277:
1992:
PICASSO Collaboration (2009). "Dark Matter Spin-Dependent Limits for WIMP Interactions on F by PICASSO".
4072:
3969:
2930:"Strong constraints from COSINE-100 on the DAMA dark matter results using the same sodium iodide target"
2843:
2256:
679:
510:
477:
Fig 1. CDMS parameter space excluded as of 2004. DAMA result is located in green area and is disallowed.
215:
192:
72:
2045:
Cooley, J. (28 October 2014). "Overview of non-liquid noble direct detection dark matter experiments".
582:, an experiment that observed an annular modulation of the signal consistent with WIMP detection (see
4704:
4576:
4344:
4092:
4014:
3929:
3890:
3817:
3770:
3684:
3678:
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3393:
3336:
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3050:
2951:
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2652:
2568:
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2350:
2184:
2122:
2064:
2011:
1925:
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1810:
1754:
1706:
1663:
1602:
1549:
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1430:
1377:
1332:
1281:
1188:
1146:
1105:
1086:
Fox, Patrick J.; Jung, Gabriel; Sorensen, Peter; Weiner, Neal (2014). "Dark matter in light of LUX".
1013:
966:
175:
Experimental efforts to detect WIMPs include the search for products of WIMP annihilation, including
4676:
4382:
1323:
Griest, Kim (1991). "Galactic Microlensing as a Method of Detecting Massive Compact Halo Objects".
834:
379:
157:{\displaystyle \langle \sigma v\rangle \simeq 3\times 10^{-26}\mathrm {cm} ^{3}\;\mathrm {s} ^{-1}}
52:
3706:
Cerdeño, David G.; Green, Anne M. (2010). Bertone, Gianfranco (ed.). "Direct detection of WIMPs".
1697:
Freese, Katherine (1986). "Can scalar neutrinos or massive Dirac neutrinos be the missing mass?".
808:
published the first results of their searches for WIMPs, the first excluding cross sections above
4664:
4652:
4097:
4057:
3875:
3807:
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2001:
1949:
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1095:
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956:
315:
60:
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Buttazzo, D.; et al. (2020). "Annual modulations from secular variations: relaxing DAMA?".
2523:
2384:
1844:
Aprile, E; et al. (2017). "First Dark Matter Search Results from the XENON1T Experiment".
690:
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2823:
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2754:
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Freese, K.; Frieman, J.; Gould, A. (1988). "Signal Modulation in Cold Dark Matter Detection".
2711:
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2200:
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1941:
1879:
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1229:
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334:
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The CDMS II Collaboration (2010). "Dark Matter Search Results from the CDMS II Experiment".
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2130:
2101:"Constraints on Light Dark Matter Particles Interacting with Electrons from DAMIC at SNOLAB"
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2019:
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68:
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4219:
3029:"An induced annual modulation signature in COSINE-100 data by DAMA/LIBRA's analysis method"
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in the laboratory, as well as attempts to directly produce WIMPs in colliders, such as the
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3939:
3609:
3543:
3371:
2100:
506:
429:
372:
3242:
3821:
3774:
3751:
Davis, Jonathan H. (2015). "The Past and Future of Light Dark Matter Direct Detection".
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2572:
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2354:
2331:
Davis, Jonathan H. (2015). "The Past and Future of Light Dark Matter Direct Detection".
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2015:
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1358:
de Swart, J. G.; Bertone, G.; van Dongen, J. (2017). "How dark matter came to matter".
1293:
994:
Jungman, Gerard; Kamionkowski, Marc; Griest, Kim (1996). "Supersymmetric dark matter".
768:
630:
355:
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188:
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with each other, theoretically forming a variety of particles, including high-energy
330:
231:
203:
3303:
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2835:
2672:
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2031:
1953:
1891:
1516:
1450:
1243:
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3643:
3577:
3405:
2774:
2580:
2508:
2389:
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2134:
2023:
1937:
1875:
1614:
1309:
912: – Neutral mass eigenstate formed from superpartners of gauge and Higgs bosons
532:
433:
294:
243:
76:
1830:
816:
at 28 GeV with 90% confidence level and the second excluding cross sections above
3725:
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instrument a very large target mass of liquid argon for sensitive WIMP searches.
4527:
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4483:
4067:
4004:
3913:
3829:
3168:
2898:
846:
659:(TPCs) filled with low pressure gases are being studied for WIMP detection. The
494:
445:
211:
45:
3295:
3107:
3062:
2444:
2076:
1791:(2008). "Status and perspectives of indirect and direct dark matter searches".
1675:
1508:
1225:
1117:
214:
experiments along with the failure to produce evidence of supersymmetry in the
4522:
4359:
4324:
4209:
4062:
4019:
3869:
3865:
3782:
2819:
2362:
2302:
1822:
1766:
1065:
Craig, Nathaniel (2013). "The State of Supersymmetry after Run I of the LHC".
909:
716:
639:
579:
565:
408:
184:
3413:
2971:
2906:
2750:
2707:
2204:
4506:
4463:
4254:
3843:
3518:
3493:
3469:
3444:
3211:
Baudis, Laura (2012). "DARWIN: dark matter WIMP search with noble liquids".
2492:
1389:
786:
have found no signal in their data, with a lowest excluded cross section of
742:
588:). Several experiments are attempting to replicate those results, including
522:
176:
3651:
3585:
3544:"First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment"
3421:
3115:
3080:
2989:
2963:
2827:
2588:
2500:
2419:
2212:
2142:
1945:
1883:
1622:
1301:
2766:
2715:
979:
944:
4214:
2535:
2257:"First Results from LUX, the World's Most Sensitive Dark Matter Detector"
1805:
1749:
1425:
772:
437:
359:
299:
268:
227:
180:
64:
44:) are hypothetical particles that are one of the proposed candidates for
1262:
Griest, Kim (1993). "The Search for the Dark Matter: WIMPs and MACHOs".
4547:
4447:
4319:
1658:
1276:
1183:
1141:
1008:
611:
420:
319:
164:, which is roughly what is expected for a new particle in the 100
59:
and any other force (or forces) which is as weak as or weaker than the
56:
3610:"First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment"
2758:
1561:
4304:
4179:
1735:; Bertone, G. (2005). "Dark Matter Dynamics and Indirect Detection".
783:
771:, while for higher masses the background contains contributions from
726:
712:
615:
569:
552:
540:
531:– Another way of detecting atoms "knocked about" by a WIMP is to use
518:
498:
351:
17:
3860:
Portraits of darkness, New Scientist, August 31, 2013. Preview only.
4635:
3765:
3626:
3560:
3388:
3151:
3045:
2946:
2881:
2802:
2345:
2291:"Largest-ever dark-matter experiment poised to test popular theory"
2179:
2117:
1858:
1442:
1372:
1344:
51:
There exists no formal definition of a WIMP, but broadly, it is an
4468:
4354:
4349:
4199:
4154:
3999:
3994:
3812:
3716:
3331:
3278:
3225:
3196:
2647:
2563:
2475:
2059:
2006:
1920:
1597:
1544:
1491:
1216:
1100:
1071:
961:
801:
619:
589:
561:
472:
3372:"Dark Matter Search Results from the PandaX-4T Commissioning Run"
3190:
Malling, D. C.; et al. (2011). "After LUX: The LZ Program".
2865:"Annual modulation results from three-year exposure of ANAIS-112"
604:
is approaching the same problem using CsI(Tl) as a scintillator.
218:(LHC) experiment has cast doubt on the simplest WIMP hypothesis.
4314:
4309:
4234:
4189:
4159:
668:
536:
263:
196:
3886:
3882:
505:(TES) are held at the critical temperature so they are in the
165:
3874:(video; colloquium). Brown University Department of Physics.
3096:"Notorious dark-matter signal could be due to analysis error"
924: – Hypothetical particle that interacts only via gravity
2235:"New Experiment Torpedoes Lightweight Dark Matter Particles"
362:, are very light, and hence would be fast moving, or "hot".
2413:"Results from the Final Exposure of the CDMS II Experiment"
859:) – Hypothetical form of dark matter in galactic halos
71:. Obtaining the correct abundance of dark matter today via
329:
Large mass compared to standard particles (WIMPs with sub-
1169:
Kamionkowski, Marc (1997). "WIMP and Axion Dark Matter".
900:) – Lightest new particle in a supersymmetric model
3708:
Particle Dark Matter: Observations, Models and Searches
3680:
Particle Dark Matter: Observations, Models and Searches
27:
Hypothetical particles that may constitute dark matter
4600:
879:
Weakly interacting sub-eV / slender / slight particle
649:
PICO is an expansion of the concept planned in 2015.
88:
310:
The main theoretical characteristics of a WIMP are:
4515:
4481:
4456:
4368:
4140:
4131:
4048:
3987:
3920:
3004:"Is the end in sight for famous dark matter claim?"
918: – Hypothetical black holes of very small size
865: – Hypothetical black holes of very small size
849: – Elementary particle involved with rest mass
715:and CRESST-II), and two which remain unexplained (
156:
3844:Particle Data Group review article on WIMP search
2612:"CoGeNT findings support dark-matter halo theory"
633:but, since only the small droplets can undergo a
3445:"Tightening the Net on Two Kinds of Dark Matter"
1906:Interactions from a Two Liter Bubble Chamber".
869:Robust associations of massive baryonic objects
3319:Journal of Cosmology and Astroparticle Physics
2635:Journal of Cosmology and Astroparticle Physics
2438:"Latest Results in the Search for Dark Matter"
2385:"Key to the universe found on the Iron Range?"
1164:
1162:
1160:
3898:
3856:in Living Reviews in Relativity, Vol 5, 2002.
2524:"A CoGeNT result in the hunt for dark matter"
661:Directional Recoil Identification From Tracks
596:, which is codeploying NaI crystals with the
8:
2278:Dark matter search comes up empty. July 2016
906: – Fermion that is its own antiparticle
98:
89:
30:"WIMPs" redirects here. For other uses, see
3683:. Cambridge University Press. p. 762.
2848:: CS1 maint: numeric names: authors list (
2259:. Berkeley Lab News Center. 30 October 2013
4137:
3905:
3891:
3883:
1264:Annals of the New York Academy of Sciences
138:
3811:
3764:
3753:International Journal of Modern Physics A
3715:
3625:
3559:
3517:
3468:
3387:
3330:
3277:
3224:
3195:
3150:
3070:
3044:
2979:
2945:
2880:
2801:
2646:
2562:
2474:
2344:
2333:International Journal of Modern Physics A
2178:
2116:
2058:
2005:
1919:
1857:
1804:
1748:
1657:
1596:
1543:
1490:
1424:
1371:
1275:
1215:
1182:
1140:
1099:
1070:
1048:"LHC discovery maims supersymmetry again"
1007:
978:
960:
618:in Canada. It uses bubble detectors with
145:
140:
132:
124:
114:
87:
1257:
1255:
1253:
753:
689:
248:
4607:
1465:Introduction: The Millennium Simulation
935:
67:cosmology, and usually will constitute
2841:
875:) – Proposed type of star cluster
797:at 40 GeV with 90% confidence level.
646:terms of spin dependent interactions.
322:, or possibly other interactions with
3871:The WIMP is dead. Long live the WIMP!
3854:Experimental Searches for Dark Matter
1206:Zacek, Viktor (2007). "Dark Matter".
824:at 36 GeV with 90% confidence level.
777:diffuse supernova neutrino background
741:2021 new results from COSINE-100 and
289:lightest Kaluza–Klein particle (LKP)
226:WIMP-like particles are predicted by
7:
4583:
2434:. See also a non-technical summary:
1135:. Vol. 1997. IOP. p. 485.
916:Planck-mass-sized black hole remnant
222:Theoretical framework and properties
38:Weakly interacting massive particles
3094:Castelvecchi, Davide (2022-08-16).
1463:The Millennium Simulation Project,
1294:10.1111/j.1749-6632.1993.tb43912.x
584:
168:mass range that interacts via the
141:
128:
125:
25:
4710:Physics beyond the Standard Model
1171:High Energy Physics and Cosmology
392:Indirect detection of dark matter
4682:
4670:
4658:
4646:
4634:
4622:
4610:
4582:
4571:
4570:
3978:
3878:from the original on 2021-12-11.
3494:"The Search for WIMPs Continues"
894:Lightest supersymmetric particle
274:lightest supersymmetric particle
3443:Stephens, Marric (2021-12-23).
837: – Hypothetical unparticle
782:In December 2021, results from
458:Direct detection of dark matter
333:masses may be considered to be
4538:Galaxy formation and evolution
3644:10.1103/PhysRevLett.131.041002
3578:10.1103/PhysRevLett.131.041003
3406:10.1103/PhysRevLett.127.261802
3243:10.1088/1742-6596/375/1/012028
3139:Journal of High Energy Physics
2581:10.1103/PhysRevLett.106.131301
2197:10.1103/PhysRevLett.122.161801
2135:10.1103/PhysRevLett.123.181802
2024:10.1016/j.physletb.2009.11.019
1968:"Bubble Technology Industries"
1938:10.1103/PhysRevLett.106.021303
1876:10.1103/PhysRevLett.119.181301
1615:10.1103/PhysRevLett.113.101101
750:The future of direct detection
326:no higher than the weak scale;
314:Interactions only through the
304:lightest T-odd particle (LTP)
1:
3349:10.1088/1475-7516/2015/03/012
2665:10.1088/1475-7516/2014/08/014
234:, a type of extension to the
3960:Self-interacting dark matter
3726:10.1017/CBO9780511770739.018
3677:Bertone, Gianfranco (2010).
2047:Physics of the Dark Universe
1719:10.1016/0370-2693(86)90349-7
1026:10.1016/0370-1573(95)00058-5
600:detector at the South Pole.
491:Cryogenic Dark Matter Search
348:massive compact halo objects
4118:Navarro–Frenk–White profile
4108:Massive compact halo object
4103:Mass dimension one fermions
3830:10.1016/j.phpro.2014.12.009
3492:Day, Charles (2023-07-28).
2899:10.1103/PhysRevD.103.102005
943:Garrett, Katherine (2010).
853:Massive compact halo object
841:Feebly interacting particle
487:Cryogenic crystal detectors
4746:
3296:10.1103/PhysRevD.89.023524
3108:10.1038/d41586-022-02222-9
3063:10.1038/s41598-023-31688-4
2610:Dacey, James (June 2011).
2077:10.1016/j.dark.2014.10.005
1793:Advances in Space Research
1676:10.1103/PhysRevD.74.115007
1532:AIP Conference Proceedings
1509:10.1103/PhysRevD.89.042001
1226:10.1142/9789812776105_0007
1118:10.1103/PhysRevD.89.103526
489:– A technique used by the
455:
413:inverse Compton scattering
389:
29:
4566:
3976:
3783:10.1142/S0217751X15300380
2820:10.1038/s41586-018-0739-1
2522:Hand, Eric (2010-02-26).
2363:10.1142/S0217751X15300380
2303:10.1038/nature.2015.18772
2289:Cartlidge, Edwin (2015).
1823:10.1016/j.asr.2007.02.067
1767:10.1142/S0217732305017391
1413:The Astrophysical Journal
1325:The Astrophysical Journal
240:universal extra dimension
4123:Scalar field dark matter
3965:Scalar field dark matter
2751:10.1103/PhysRevD.37.3388
2708:10.1103/PhysRevD.33.3495
1737:Modern Physics Letters A
1208:Fundamental Interactions
657:Time projection chambers
653:Other types of detectors
3614:Physical Review Letters
3548:Physical Review Letters
3519:10.1103/Physics.16.s106
3470:10.1103/Physics.14.s164
3376:Physical Review Letters
3169:10.1007/JHEP04(2020)137
2551:Physical Review Letters
2493:10.1126/science.1186112
2167:Physical Review Letters
2105:Physical Review Letters
1908:Physical Review Letters
1846:Physical Review Letters
1585:Physical Review Letters
1390:10.1038/s41550-017-0059
945:"Dark matter: A primer"
529:Noble gas scintillators
503:transition edge sensors
493:(CDMS) detector at the
482:Experimental techniques
4725:Hypothetical particles
3988:Hypothetical particles
3970:Primordial black holes
2964:10.1126/sciadv.abk2699
887:Theoretical candidates
759:
696:
680:Charge Coupled Devices
478:
158:
32:WIMPS (disambiguation)
4715:Astroparticle physics
4073:Dark globular cluster
949:Advances in Astronomy
773:atmospheric neutrinos
757:
693:
576:Crystal scintillators
476:
216:Large Hadron Collider
193:Large Hadron Collider
159:
4093:Dwarf galaxy problem
4015:Minicharged particle
3930:Baryonic dark matter
2536:10.1038/news.2010.97
2436:CDMS Collaboration.
2411:CDMS Collaboration.
585:§ Recent limits
525:run similar setups.
86:
55:which interacts via
4730:Physics experiments
3822:2015PhPro..61...45D
3775:2015IJMPA..3030038D
3689:2010pdmo.book.....B
3636:2023PhRvL.131d1002A
3570:2023PhRvL.131d1003A
3510:2023PhyOJ..16.s106D
3461:2021PhyOJ..14.s164S
3398:2021PhRvL.127z1802M
3341:2015JCAP...03..012D
3288:2014PhRvD..89b3524B
3235:2012JPhCS.375a2028B
3161:2020JHEP...04..137B
3055:2023NatSR..13.4676A
2956:2021SciA....7.2699A
2891:2021PhRvD.103j2005A
2812:2018Natur.564...83C
2743:1988PhRvD..37.3388F
2700:1986PhRvD..33.3495D
2657:2014JCAP...08..014D
2573:2011PhRvL.106m1301A
2485:2010Sci...327.1619C
2469:(5973): 1619–1621.
2355:2015IJMPA..3030038D
2189:2019PhRvL.122p1801A
2127:2019PhRvL.123r1802A
2069:2014PDU.....4...92C
2016:2009PhLB..682..185A
1930:2011PhRvL.106b1303B
1868:2017PhRvL.119r1301A
1815:2008AdSpR..41.2010F
1759:2005MPLA...20.1021B
1711:1986PhLB..167..295F
1668:2006PhRvD..74k5007F
1607:2014PhRvL.113j1101A
1554:2012AIPC.1505..689G
1501:2014PhRvD..89d2001A
1435:2006ApJ...647..201C
1382:2017NatAs...1E..59D
1337:1991ApJ...366..412G
1286:1993NYASA.688..390G
1193:1998hepc.conf..394K
1151:1998hep.ex....2007K
1110:2014PhRvD..89j3526F
1018:1996PhR...267..195J
980:10.1155/2011/968283
971:2011AdAst2011E...8G
835:Darkon (unparticle)
380:thermal equilibrium
346:, the others being
53:elementary particle
4098:Halo mass function
4058:Cuspy halo problem
3213:J. Phys. Conf. Ser
3033:Scientific Reports
760:
697:
479:
404:satellite galaxies
399:Indirect detection
386:Indirect detection
316:weak nuclear force
154:
73:thermal production
61:weak nuclear force
4598:
4597:
4543:Illustris project
4477:
4476:
3950:Mixed dark matter
3945:Light dark matter
3868:(13 April 2018).
3850:Timothy J. Sumner
3698:978-0-521-76368-4
3266:Physical Review D
2869:Physical Review D
2737:(12): 3388–3405.
2731:Physical Review D
2694:(12): 3495–3508.
2688:Physical Review D
2237:. 30 October 2013
1994:Physics Letters B
1799:(12): 2010–2018.
1789:Fornengo, Nicolao
1743:(14): 1021–1036.
1699:Physics Letters B
1646:Physical Review D
1562:10.1063/1.4772353
1479:Physical Review D
1235:978-981-277-609-9
1133:Beyond the Desert
1088:Physical Review D
800:In July 2023 the
335:light dark matter
308:
307:
170:electroweak force
16:(Redirected from
4737:
4687:
4686:
4675:
4674:
4673:
4663:
4662:
4661:
4651:
4650:
4649:
4639:
4638:
4627:
4626:
4625:
4615:
4614:
4606:
4586:
4585:
4574:
4573:
4138:
4078:Dark matter halo
4025:Sterile neutrino
3982:
3981:
3955:Warm dark matter
3935:Cold dark matter
3907:
3900:
3893:
3884:
3879:
3833:
3815:
3800:Physics Procedia
3794:
3768:
3747:
3719:
3702:
3664:
3663:
3629:
3604:
3598:
3597:
3563:
3538:
3532:
3531:
3521:
3489:
3483:
3482:
3472:
3440:
3434:
3433:
3391:
3367:
3361:
3360:
3334:
3314:
3308:
3307:
3281:
3261:
3255:
3254:
3228:
3208:
3202:
3201:
3199:
3187:
3181:
3180:
3154:
3134:
3128:
3127:
3091:
3085:
3084:
3074:
3048:
3024:
3018:
3017:
3015:
3014:
3000:
2994:
2993:
2983:
2949:
2940:(46): eabk2699.
2934:Science Advances
2925:
2919:
2918:
2884:
2860:
2854:
2853:
2847:
2839:
2805:
2785:
2779:
2778:
2726:
2720:
2719:
2683:
2677:
2676:
2650:
2630:
2624:
2623:
2621:
2619:
2607:
2601:
2600:
2566:
2546:
2540:
2539:
2519:
2513:
2512:
2478:
2458:
2452:
2451:
2449:
2443:. Archived from
2442:
2433:
2431:
2430:
2424:
2418:. Archived from
2417:
2408:
2402:
2401:
2399:
2397:
2381:
2375:
2374:
2348:
2328:
2322:
2321:
2319:
2317:
2286:
2280:
2275:
2269:
2268:
2266:
2264:
2253:
2247:
2246:
2244:
2242:
2231:
2225:
2224:
2182:
2161:
2155:
2154:
2120:
2095:
2089:
2088:
2062:
2042:
2036:
2035:
2009:
1989:
1983:
1982:
1980:
1979:
1970:. Archived from
1964:
1958:
1957:
1923:
1902:
1896:
1895:
1861:
1841:
1835:
1834:
1808:
1806:astro-ph/0612786
1785:
1779:
1778:
1752:
1750:astro-ph/0504422
1729:
1723:
1722:
1694:
1688:
1687:
1661:
1641:
1635:
1634:
1600:
1580:
1574:
1573:
1547:
1527:
1521:
1520:
1494:
1474:
1468:
1461:
1455:
1454:
1428:
1426:astro-ph/0512234
1408:
1402:
1401:
1375:
1360:Nature Astronomy
1355:
1349:
1348:
1320:
1314:
1313:
1279:
1259:
1248:
1247:
1219:
1203:
1197:
1196:
1186:
1166:
1155:
1154:
1144:
1128:
1122:
1121:
1103:
1083:
1077:
1076:
1074:
1062:
1056:
1055:
1044:
1038:
1037:
1011:
1002:(5–6): 195–373.
991:
985:
984:
982:
964:
955:(968283): 1–22.
940:
922:Sterile neutrino
904:Majorana fermion
899:
874:
863:Micro black hole
858:
823:
821:
815:
813:
796:
791:
665:carbon disulfide
635:phase transition
572:collaborations.
463:Direct detection
452:Direct detection
442:Super-Kamiokande
344:cold dark matter
249:
212:direct-detection
163:
161:
160:
155:
153:
152:
144:
137:
136:
131:
122:
121:
75:requires a self-
69:cold dark matter
21:
4745:
4744:
4740:
4739:
4738:
4736:
4735:
4734:
4695:
4694:
4693:
4681:
4671:
4669:
4659:
4657:
4647:
4645:
4633:
4623:
4621:
4609:
4601:
4599:
4594:
4562:
4558:UniverseMachine
4511:
4473:
4452:
4370:
4364:
4142:
4133:
4127:
4050:
4044:
3983:
3979:
3974:
3940:Hot dark matter
3922:
3916:
3911:
3864:
3840:
3797:
3759:(15): 1530038.
3750:
3736:
3705:
3699:
3676:
3673:
3671:Further reading
3668:
3667:
3606:
3605:
3601:
3540:
3539:
3535:
3491:
3490:
3486:
3442:
3441:
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3364:
3316:
3315:
3311:
3263:
3262:
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3210:
3209:
3205:
3189:
3188:
3184:
3136:
3135:
3131:
3093:
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3088:
3026:
3025:
3021:
3012:
3010:
3008:www.science.org
3002:
3001:
2997:
2927:
2926:
2922:
2862:
2861:
2857:
2840:
2796:(7734): 83–86.
2787:
2786:
2782:
2728:
2727:
2723:
2685:
2684:
2680:
2632:
2631:
2627:
2617:
2615:
2609:
2608:
2604:
2548:
2547:
2543:
2530:. Nature News.
2521:
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2426:
2422:
2415:
2410:
2409:
2405:
2395:
2393:
2383:
2382:
2378:
2339:(15): 1530038.
2330:
2329:
2325:
2315:
2313:
2288:
2287:
2283:
2276:
2272:
2262:
2260:
2255:
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2240:
2238:
2233:
2232:
2228:
2163:
2162:
2158:
2097:
2096:
2092:
2044:
2043:
2039:
1991:
1990:
1986:
1977:
1975:
1966:
1965:
1961:
1904:
1903:
1899:
1843:
1842:
1838:
1787:
1786:
1782:
1731:
1730:
1726:
1696:
1695:
1691:
1643:
1642:
1638:
1582:
1581:
1577:
1529:
1528:
1524:
1476:
1475:
1471:
1462:
1458:
1410:
1409:
1405:
1357:
1356:
1352:
1322:
1321:
1317:
1261:
1260:
1251:
1236:
1205:
1204:
1200:
1168:
1167:
1158:
1130:
1129:
1125:
1085:
1084:
1080:
1064:
1063:
1059:
1046:
1045:
1041:
996:Physics Reports
993:
992:
988:
942:
941:
937:
932:
927:
897:
884:
872:
856:
830:
819:
817:
811:
809:
789:
787:
752:
688:
674:
625:
608:Bubble chambers
507:superconducting
484:
460:
454:
430:escape velocity
394:
388:
373:hot dark matter
368:
224:
139:
123:
110:
84:
83:
35:
28:
23:
22:
15:
12:
11:
5:
4743:
4741:
4733:
4732:
4727:
4722:
4717:
4712:
4707:
4697:
4696:
4692:
4691:
4679:
4667:
4655:
4643:
4631:
4619:
4596:
4595:
4593:
4592:
4580:
4567:
4564:
4563:
4561:
4560:
4555:
4550:
4548:Imaginary mass
4545:
4540:
4535:
4530:
4525:
4519:
4517:
4513:
4512:
4510:
4509:
4504:
4499:
4497:HVC 127-41-330
4494:
4488:
4486:
4479:
4478:
4475:
4474:
4472:
4471:
4466:
4460:
4458:
4457:Other projects
4454:
4453:
4451:
4450:
4445:
4440:
4435:
4430:
4425:
4420:
4415:
4410:
4405:
4400:
4395:
4390:
4385:
4380:
4374:
4372:
4366:
4365:
4363:
4362:
4357:
4352:
4347:
4342:
4337:
4332:
4327:
4322:
4317:
4312:
4307:
4302:
4297:
4292:
4287:
4282:
4277:
4272:
4267:
4262:
4257:
4252:
4247:
4242:
4237:
4232:
4227:
4222:
4217:
4212:
4207:
4202:
4197:
4192:
4187:
4182:
4177:
4172:
4167:
4162:
4157:
4152:
4146:
4144:
4135:
4129:
4128:
4126:
4125:
4120:
4115:
4110:
4105:
4100:
4095:
4090:
4085:
4083:Dark radiation
4080:
4075:
4070:
4065:
4060:
4054:
4052:
4046:
4045:
4043:
4042:
4037:
4032:
4027:
4022:
4017:
4012:
4007:
4002:
3997:
3991:
3989:
3985:
3984:
3977:
3975:
3973:
3972:
3967:
3962:
3957:
3952:
3947:
3942:
3937:
3932:
3926:
3924:
3918:
3917:
3912:
3910:
3909:
3902:
3895:
3887:
3881:
3880:
3862:
3857:
3847:
3839:
3838:External links
3836:
3835:
3834:
3795:
3748:
3734:
3703:
3697:
3672:
3669:
3666:
3665:
3599:
3533:
3484:
3435:
3382:(26): 261802.
3362:
3309:
3256:
3203:
3182:
3129:
3086:
3019:
2995:
2920:
2875:(10): 102005.
2855:
2780:
2721:
2678:
2625:
2614:. physicsworld
2602:
2557:(13): 131301.
2541:
2514:
2453:
2450:on 2010-06-18.
2403:
2376:
2323:
2281:
2270:
2248:
2226:
2173:(16): 161801.
2165:Skipper-CCD".
2156:
2111:(18): 181802.
2090:
2037:
2000:(2): 185–192.
1984:
1959:
1897:
1852:(18): 181301.
1836:
1780:
1724:
1705:(3): 295–300.
1689:
1659:hep-ph/0609257
1652:(11): 115007.
1636:
1591:(10): 101101.
1575:
1522:
1469:
1456:
1443:10.1086/503602
1419:(1): 201–214.
1403:
1350:
1345:10.1086/169575
1315:
1277:hep-ph/9303253
1249:
1234:
1198:
1184:hep-ph/9710467
1156:
1142:hep-ex/9802007
1123:
1094:(10): 103526.
1078:
1057:
1052:Discovery News
1039:
1009:hep-ph/9506380
986:
934:
933:
931:
928:
926:
925:
919:
913:
907:
901:
890:
889:
888:
883:
882:
876:
866:
860:
850:
844:
838:
831:
829:
826:
751:
748:
687:
684:
672:
631:bubble chamber
623:
483:
480:
453:
450:
387:
384:
367:
366:As dark matter
364:
356:Standard Model
339:
338:
327:
324:cross-sections
306:
305:
302:
297:
291:
290:
287:
284:
278:
277:
271:
266:
260:
259:
256:
253:
236:Standard Model
223:
220:
204:supersymmetric
151:
148:
143:
135:
130:
127:
120:
117:
113:
109:
106:
103:
100:
97:
94:
91:
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
4742:
4731:
4728:
4726:
4723:
4721:
4720:Exotic matter
4718:
4716:
4713:
4711:
4708:
4706:
4703:
4702:
4700:
4690:
4685:
4680:
4678:
4668:
4666:
4656:
4654:
4644:
4642:
4637:
4632:
4630:
4620:
4618:
4613:
4608:
4604:
4591:
4590:
4581:
4579:
4578:
4569:
4568:
4565:
4559:
4556:
4554:
4553:Negative mass
4551:
4549:
4546:
4544:
4541:
4539:
4536:
4534:
4533:Exotic matter
4531:
4529:
4526:
4524:
4521:
4520:
4518:
4514:
4508:
4505:
4503:
4502:Smith's Cloud
4500:
4498:
4495:
4493:
4490:
4489:
4487:
4485:
4484:dark galaxies
4480:
4470:
4467:
4465:
4462:
4461:
4459:
4455:
4449:
4446:
4444:
4441:
4439:
4436:
4434:
4431:
4429:
4426:
4424:
4421:
4419:
4416:
4414:
4411:
4409:
4406:
4404:
4401:
4399:
4396:
4394:
4391:
4389:
4386:
4384:
4381:
4379:
4376:
4375:
4373:
4367:
4361:
4358:
4356:
4353:
4351:
4348:
4346:
4343:
4341:
4338:
4336:
4333:
4331:
4328:
4326:
4323:
4321:
4318:
4316:
4313:
4311:
4308:
4306:
4303:
4301:
4298:
4296:
4293:
4291:
4288:
4286:
4283:
4281:
4278:
4276:
4273:
4271:
4268:
4266:
4263:
4261:
4258:
4256:
4253:
4251:
4248:
4246:
4243:
4241:
4238:
4236:
4233:
4231:
4228:
4226:
4223:
4221:
4218:
4216:
4213:
4211:
4208:
4206:
4203:
4201:
4198:
4196:
4193:
4191:
4188:
4186:
4183:
4181:
4178:
4176:
4173:
4171:
4168:
4166:
4163:
4161:
4158:
4156:
4153:
4151:
4148:
4147:
4145:
4139:
4136:
4130:
4124:
4121:
4119:
4116:
4114:
4113:Mirror matter
4111:
4109:
4106:
4104:
4101:
4099:
4096:
4094:
4091:
4089:
4086:
4084:
4081:
4079:
4076:
4074:
4071:
4069:
4066:
4064:
4061:
4059:
4056:
4055:
4053:
4047:
4041:
4038:
4036:
4033:
4031:
4028:
4026:
4023:
4021:
4018:
4016:
4013:
4011:
4008:
4006:
4003:
4001:
3998:
3996:
3993:
3992:
3990:
3986:
3971:
3968:
3966:
3963:
3961:
3958:
3956:
3953:
3951:
3948:
3946:
3943:
3941:
3938:
3936:
3933:
3931:
3928:
3927:
3925:
3919:
3915:
3908:
3903:
3901:
3896:
3894:
3889:
3888:
3885:
3877:
3873:
3872:
3867:
3863:
3861:
3858:
3855:
3851:
3848:
3845:
3842:
3841:
3837:
3831:
3827:
3823:
3819:
3814:
3809:
3805:
3801:
3796:
3792:
3788:
3784:
3780:
3776:
3772:
3767:
3762:
3758:
3754:
3749:
3745:
3741:
3737:
3735:9780511770739
3731:
3727:
3723:
3718:
3713:
3709:
3704:
3700:
3694:
3690:
3686:
3682:
3681:
3675:
3674:
3670:
3661:
3657:
3653:
3649:
3645:
3641:
3637:
3633:
3628:
3623:
3620:(4): 041002.
3619:
3615:
3611:
3603:
3600:
3595:
3591:
3587:
3583:
3579:
3575:
3571:
3567:
3562:
3557:
3554:(4): 041003.
3553:
3549:
3545:
3537:
3534:
3529:
3525:
3520:
3515:
3511:
3507:
3503:
3499:
3495:
3488:
3485:
3480:
3476:
3471:
3466:
3462:
3458:
3454:
3450:
3446:
3439:
3436:
3431:
3427:
3423:
3419:
3415:
3411:
3407:
3403:
3399:
3395:
3390:
3385:
3381:
3377:
3373:
3366:
3363:
3358:
3354:
3350:
3346:
3342:
3338:
3333:
3328:
3324:
3320:
3313:
3310:
3305:
3301:
3297:
3293:
3289:
3285:
3280:
3275:
3272:(2): 023524.
3271:
3267:
3260:
3257:
3252:
3248:
3244:
3240:
3236:
3232:
3227:
3222:
3219:(1): 012028.
3218:
3214:
3207:
3204:
3198:
3193:
3186:
3183:
3178:
3174:
3170:
3166:
3162:
3158:
3153:
3148:
3144:
3140:
3133:
3130:
3125:
3121:
3117:
3113:
3109:
3105:
3101:
3097:
3090:
3087:
3082:
3078:
3073:
3068:
3064:
3060:
3056:
3052:
3047:
3042:
3038:
3034:
3030:
3023:
3020:
3009:
3005:
2999:
2996:
2991:
2987:
2982:
2977:
2973:
2969:
2965:
2961:
2957:
2953:
2948:
2943:
2939:
2935:
2931:
2924:
2921:
2916:
2912:
2908:
2904:
2900:
2896:
2892:
2888:
2883:
2878:
2874:
2870:
2866:
2859:
2856:
2851:
2845:
2837:
2833:
2829:
2825:
2821:
2817:
2813:
2809:
2804:
2799:
2795:
2791:
2784:
2781:
2776:
2772:
2768:
2764:
2760:
2756:
2752:
2748:
2744:
2740:
2736:
2732:
2725:
2722:
2717:
2713:
2709:
2705:
2701:
2697:
2693:
2689:
2682:
2679:
2674:
2670:
2666:
2662:
2658:
2654:
2649:
2644:
2640:
2636:
2629:
2626:
2613:
2606:
2603:
2598:
2594:
2590:
2586:
2582:
2578:
2574:
2570:
2565:
2560:
2556:
2552:
2545:
2542:
2537:
2533:
2529:
2525:
2518:
2515:
2510:
2506:
2502:
2498:
2494:
2490:
2486:
2482:
2477:
2472:
2468:
2464:
2457:
2454:
2446:
2439:
2425:on 2009-12-29
2421:
2414:
2407:
2404:
2392:
2391:
2386:
2380:
2377:
2372:
2368:
2364:
2360:
2356:
2352:
2347:
2342:
2338:
2334:
2327:
2324:
2312:
2308:
2304:
2300:
2296:
2292:
2285:
2282:
2279:
2274:
2271:
2258:
2252:
2249:
2236:
2230:
2227:
2222:
2218:
2214:
2210:
2206:
2202:
2198:
2194:
2190:
2186:
2181:
2176:
2172:
2168:
2160:
2157:
2152:
2148:
2144:
2140:
2136:
2132:
2128:
2124:
2119:
2114:
2110:
2106:
2102:
2094:
2091:
2086:
2082:
2078:
2074:
2070:
2066:
2061:
2056:
2052:
2048:
2041:
2038:
2033:
2029:
2025:
2021:
2017:
2013:
2008:
2003:
1999:
1995:
1988:
1985:
1974:on 2008-03-20
1973:
1969:
1963:
1960:
1955:
1951:
1947:
1943:
1939:
1935:
1931:
1927:
1922:
1917:
1914:(2): 021303.
1913:
1909:
1901:
1898:
1893:
1889:
1885:
1881:
1877:
1873:
1869:
1865:
1860:
1855:
1851:
1847:
1840:
1837:
1832:
1828:
1824:
1820:
1816:
1812:
1807:
1802:
1798:
1794:
1790:
1784:
1781:
1776:
1772:
1768:
1764:
1760:
1756:
1751:
1746:
1742:
1738:
1734:
1728:
1725:
1720:
1716:
1712:
1708:
1704:
1700:
1693:
1690:
1685:
1681:
1677:
1673:
1669:
1665:
1660:
1655:
1651:
1647:
1640:
1637:
1632:
1628:
1624:
1620:
1616:
1612:
1608:
1604:
1599:
1594:
1590:
1586:
1579:
1576:
1571:
1567:
1563:
1559:
1555:
1551:
1546:
1541:
1537:
1533:
1526:
1523:
1518:
1514:
1510:
1506:
1502:
1498:
1493:
1488:
1485:(4): 042001.
1484:
1480:
1473:
1470:
1466:
1460:
1457:
1452:
1448:
1444:
1440:
1436:
1432:
1427:
1422:
1418:
1414:
1407:
1404:
1399:
1395:
1391:
1387:
1383:
1379:
1374:
1369:
1365:
1361:
1354:
1351:
1346:
1342:
1338:
1334:
1330:
1326:
1319:
1316:
1311:
1307:
1303:
1299:
1295:
1291:
1287:
1283:
1278:
1273:
1269:
1265:
1258:
1256:
1254:
1250:
1245:
1241:
1237:
1231:
1227:
1223:
1218:
1213:
1209:
1202:
1199:
1194:
1190:
1185:
1180:
1176:
1172:
1165:
1163:
1161:
1157:
1152:
1148:
1143:
1138:
1134:
1127:
1124:
1119:
1115:
1111:
1107:
1102:
1097:
1093:
1089:
1082:
1079:
1073:
1068:
1061:
1058:
1053:
1049:
1043:
1040:
1035:
1031:
1027:
1023:
1019:
1015:
1010:
1005:
1001:
997:
990:
987:
981:
976:
972:
968:
963:
958:
954:
950:
946:
939:
936:
929:
923:
920:
917:
914:
911:
908:
905:
902:
895:
892:
891:
886:
885:
880:
877:
870:
867:
864:
861:
854:
851:
848:
845:
842:
839:
836:
833:
832:
827:
825:
807:
806:LZ experiment
803:
798:
795:
785:
780:
778:
774:
770:
764:
756:
749:
747:
744:
739:
734:
730:
728:
724:
722:
718:
714:
709:
706:
702:
692:
686:Recent limits
685:
683:
681:
676:
670:
666:
662:
658:
654:
650:
647:
643:
641:
636:
632:
627:
621:
617:
613:
609:
605:
603:
599:
595:
591:
587:
586:
581:
577:
573:
571:
567:
563:
558:
554:
550:
546:
542:
538:
534:
533:scintillating
530:
526:
524:
520:
516:
512:
508:
504:
500:
496:
492:
488:
481:
475:
471:
467:
464:
459:
451:
449:
447:
443:
439:
435:
431:
425:
422:
418:
414:
410:
405:
400:
393:
385:
383:
381:
376:
374:
365:
363:
361:
357:
353:
350:(MACHOs) and
349:
345:
336:
332:
328:
325:
321:
317:
313:
312:
311:
303:
301:
298:
296:
293:
292:
288:
285:
283:
280:
279:
275:
272:
270:
267:
265:
262:
261:
257:
254:
251:
250:
247:
245:
241:
237:
233:
232:supersymmetry
229:
221:
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2390:Star Tribune
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369:
340:
309:
295:little Higgs
244:little Higgs
230:-conserving
225:
208:WIMP miracle
207:
201:
174:
77:annihilation
50:
41:
37:
36:
4705:Dark matter
4665:Outer space
4653:Spaceflight
4528:Dark energy
4492:HE0450-2958
4134:experiments
4068:Dark galaxy
4051:and objects
4005:Dark photon
3923:dark matter
3914:Dark matter
3866:Hooper, Dan
3710:: 347–369.
3039:(1): 4676.
1733:Merritt, D.
1538:: 689–692.
1331:: 412–421.
1270:: 390–407.
1210:: 170–206.
847:Higgs boson
495:Soudan Mine
446:Higgs boson
185:cosmic rays
46:dark matter
4699:Categories
4523:Antimatter
4482:Potential
4210:DAMA/LIBRA
4063:Dark fluid
4020:Neutralino
3766:1506.03924
3627:2207.03764
3561:2303.14729
3389:2107.13438
3325:(3): 012.
3152:2002.00459
3145:(4): 137.
3046:2208.05158
3013:2021-12-29
2947:2104.03537
2882:2103.01175
2803:1906.01791
2641:(8): 014.
2429:2009-12-21
2346:1506.03924
2316:15 January
2180:1901.10478
2118:1907.12628
1978:2010-03-16
1859:1705.06655
1373:1703.00013
930:References
910:Neutralino
822:10 cm
814:10 cm
738:COSINE-100
717:DAMA/LIBRA
580:DAMA/LIBRA
566:LUX-ZEPLIN
511:resistance
456:See also:
434:annihilate
409:gamma rays
390:See also:
286:KK-parity
258:candidate
246:theories.
177:gamma rays
4629:Astronomy
4507:VIRGOHI21
4464:MultiDark
4371:detection
4255:EDELWEISS
4143:detection
4088:Dark star
3813:1405.5582
3806:: 45–54.
3791:119269304
3744:119311963
3717:1002.1912
3660:250343331
3594:257767449
3528:260751963
3479:247277808
3430:236469421
3414:0031-9007
3357:118596203
3332:1412.1475
3279:1307.5458
3226:1201.2402
3197:1110.0103
3177:211010848
3124:251624302
2972:2375-2548
2915:232092298
2907:2470-0010
2648:1405.0495
2564:1002.4703
2476:0912.3592
2371:119269304
2311:182831370
2221:119219165
2205:0031-9007
2151:198985735
2085:118724305
2060:1410.4960
2053:: 92–97.
2007:0907.0307
1921:1008.3518
1775:119405319
1684:119351935
1631:220469354
1598:1405.5303
1570:118510709
1545:1210.4961
1492:1310.0828
1398:119092226
1217:0707.0472
1101:1401.0216
1072:1309.0528
1034:119067698
962:1006.2483
743:ANAIS-112
705:SuperCDMS
523:EDELWEISS
438:neutrinos
360:neutrinos
181:neutrinos
147:−
116:−
108:×
102:≃
99:⟩
93:σ
90:⟨
4577:Category
4369:Indirect
4225:DarkSide
4215:DAMA/NaI
4049:Theories
3921:Forms of
3876:Archived
3652:37566836
3586:37566859
3504:: s106.
3422:35029500
3304:16208132
3251:30885844
3116:35974221
3081:36949218
3072:10033922
2990:34757778
2836:54459495
2828:30518890
2673:54532870
2597:24822628
2589:21517370
2501:20150446
2213:31075006
2143:31763884
2032:15163629
1954:20188890
1946:21405218
1892:45532100
1884:29219593
1623:25238345
1517:46664722
1451:13189513
1302:26469437
1244:16734425
828:See also
792:10
775:and the
545:DarkSide
300:T-parity
269:R-parity
228:R-parity
202:Because
65:Big Bang
4689:Science
4617:Physics
4603:Portals
4589:Commons
4516:Related
4448:VERITAS
4423:IceCube
4383:ANTARES
4335:TREX-DM
4320:ROSEBUD
4310:PICASSO
3818:Bibcode
3771:Bibcode
3685:Bibcode
3632:Bibcode
3566:Bibcode
3506:Bibcode
3498:Physics
3457:Bibcode
3449:Physics
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2981:8580298
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2767:9958634
2759:1448427
2739:Bibcode
2716:9956575
2696:Bibcode
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2509:2517711
2481:Bibcode
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2123:Bibcode
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2012:Bibcode
1926:Bibcode
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1378:Bibcode
1333:Bibcode
1310:8955141
1282:Bibcode
1189:Bibcode
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1147:Bibcode
1106:Bibcode
1014:Bibcode
967:Bibcode
802:XENONnT
721:CDMS-Si
612:PICASSO
598:IceCube
547:at the
421:IceCube
320:gravity
255:parity
57:gravity
4443:PAMELA
4378:AMS-02
4360:ZEPLIN
4330:SIMPLE
4305:PandaX
4300:NEWS-G
4295:NEWAGE
4260:EURECA
4240:DM-Ice
4230:DARWIN
4195:CRESST
4185:COSINE
4180:CoGeNT
4141:Direct
4132:Search
3789:
3742:
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873:RAMBOs
784:PandaX
727:CoGeNT
713:CoGeNT
708:2016.
640:SIMPLE
616:SNOLAB
610:– The
594:DM-Ice
570:PandaX
555:, and
553:ZEPLIN
541:SNOLAB
521:, and
519:CoGeNT
515:CRESST
352:axions
276:(LSP)
252:Model
189:nuclei
4641:Stars
4469:PVLAS
4428:MAGIC
4408:Fermi
4403:DAMPE
4393:CALET
4355:XMASS
4350:XENON
4340:UKDMC
4325:SABRE
4290:NAIAD
4285:MIMAC
4280:MACRO
4250:DRIFT
4245:DMTPC
4220:DAMIC
4200:CUORE
4190:COUPP
4175:CLEAN
4155:ANAIS
4000:Axion
3995:Axino
3808:arXiv
3787:S2CID
3761:arXiv
3740:S2CID
3712:arXiv
3656:S2CID
3622:arXiv
3590:S2CID
3556:arXiv
3524:S2CID
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3192:arXiv
3173:S2CID
3147:arXiv
3120:S2CID
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2798:arXiv
2771:S2CID
2669:S2CID
2643:arXiv
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2593:S2CID
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1950:S2CID
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1888:S2CID
1854:arXiv
1827:S2CID
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1680:S2CID
1654:arXiv
1627:S2CID
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1566:S2CID
1540:arXiv
1513:S2CID
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1421:arXiv
1394:S2CID
1368:arXiv
1306:S2CID
1272:arXiv
1240:S2CID
1212:arXiv
1179:arXiv
1137:arXiv
1096:arXiv
1067:arXiv
1030:S2CID
1004:arXiv
957:arXiv
857:MACHO
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675:gas.
620:Freon
590:ANAIS
562:XENON
557:XENON
417:Fermi
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18:WIMPs
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4418:HESS
4413:HAWC
4398:CAST
4388:ATIC
4345:WARP
4315:PICO
4265:KIMS
4235:DEAP
4170:CDMS
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4160:ArDM
4150:ADMX
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3730:ISBN
3693:ISBN
3648:PMID
3582:PMID
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3143:2020
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2763:PMID
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2620:2015
2585:PMID
2497:PMID
2398:2009
2318:2017
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1619:PMID
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543:and
537:DEAP
318:and
264:SUSY
242:and
197:CERN
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